University of Arkansas, Fayetteville ScholarWorks@UARK Theses and Dissertations 12-2012 Exploring the Surface Liquid and Lake Regions of Titan with Laboratory Experimentation and Cassini Spacecraft aD ta Felix Casimir Wasiak University of Arkansas, Fayetteville Follow this and additional works at: http://scholarworks.uark.edu/etd Part of the Hydrology Commons, Stars, Interstellar Medium and the Galaxy Commons, and the The unS and the Solar System Commons Recommended Citation Wasiak, Felix Casimir, "Exploring the Surface Liquid and Lake Regions of Titan with Laboratory Experimentation and Cassini Spacecraft aD ta" (2012). Theses and Dissertations. 572. http://scholarworks.uark.edu/etd/572 This Dissertation is brought to you for free and open access by ScholarWorks@UARK. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of ScholarWorks@UARK. For more information, please contact [email protected], [email protected]. EXPLORING THE SURFACE LIQUID AND LAKE REGIONS OF TITAN WITH LABORATORY EXPERIMENTATION AND CASSINI SPACECRAFT DATA EXPLORING THE SURFACE LIQUID AND LAKE REGIONS OF TITAN WITH LABORATORY EXPERIMENTATION AND CASSINI SPACECRAFT DATA A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Space and Planetary Sciences By Felix C. Wasiak State University of New York College at Buffalo Bachelor of Technology, 1982 December 2012 University of Arkansas ABSTRACT The surface liquids and lake regions of Titan are studied utilizing three unique techniques, the results of which are reported in this dissertation. The development of a facility to simulate the surface conditions of Titan, and to conduct experiments on samples within that facility, brings an understanding of Titan’s surface not possible through observation and modeling alone. The properties of this facility are presented, including conceptual methodology, design, implementation, performance, and experimental results. The facility, the main component of which is a simulation chamber, allows for Titan temperatures of 90 – 94 K and a 1.5 bar N2 atmosphere. The sample cryogenic liquids or ice undergoing experimentation are condensed within the chamber itself. During experiments, evaporation rates are determined by directly measuring mass, while vapor concentrations are determined using a gas chromatograph fitted with a flame ionization detector. The infrared (IR) spectra of liquid and ice constituents are analyzed with a Fourier transform infrared spectroscopy spectrometer (FTIR) via a fiber optic probe, and all pertinent data is logged in a computer. With the Cassini spacecraft currently orbiting Saturn and conducting periodic close flybys of Titan, a unique opportunity exists to search for change in lake size and shorelines in the northern lake region due to the temporally spaced overlapping data coverage. The results of a Geographic Information System (GIS) approach to monitoring Titan’s northern lakes for change found no discernible change in northern lake size or shorelines over a 32 month period. GIS analysis of an estuary of Kraken Mare, for synthetic aperture radar (SAR) swaths taken 47 days apart, indicate a transient feature, with implications for short-term dynamic processes. A geological characterization of Ligeia Mare, the second largest sea on Titan, was performed utilizing Cassini SAR swaths. SAR swaths were mosaicked, and the mosaic interpreted so as to identify the principle components of the surrounding terrain. Interpretations related to landscape forming processes were formulated, measurements of drainage channel directions and the areal extent of main channels and tributaries are reported, and the sediment volume that has flowed into Ligeia through time is estimated. This dissertation is approved for recommendation to the Graduate Council. Dissertation Director: _________________________________________ Dr. Vincent F. Chevrier Dissertation Committee: _________________________________________ Dr. Daniel Kennefick _________________________________________ Dr. John Dixon _________________________________________ Dr. Jason A. Tullis _________________________________________ Dr. Mack Ivey _________________________________________ Dr. Michael Lieber DISSERTATION DUPLICATION RELEASE I hereby authorize the University of Arkansas Libraries to duplicate this dissertation when needed for research and/or scholarship. Agreed _______________________________________________ Felix C. Wasiak Refused _______________________________________________ Felix C. Wasiak TABLE OF CONTENTS I. INTRODUCTION A. Saturn's Moon Titan 1. Discovery 2. Gravitational Force 3. Solar Heating 4. Lakes 5. Atmosphere a. Thermal Profile b. Composition c. Properties of the Atmosphere d. Haze and Clouds e. Super-Rotation and Winds f. The Greenhouse and Anti-Greenhouse Effects g. Methane Sources and Sinks 6. Surface 7. Interior 8. Formation B. Radar Remote Sensing 1. Cassini’s Radar 2. Synthetic Aperture Radar Imaging of Titan’s Surface and Lakes 3. Space-Borne Radar in the Exploration of the Solar System C. Titan's Hydrology D. Questions Addressed By This Study 1. Science Questions 2. Engineering Questions E. Outline of Chapters F. References II. A FACILITY FOR SIMULATING TITAN’S ENVIRONMENT A. Abstract B. Introduction C. Methods 1. Andromeda Simulation Chamber 2. Titan Module 3. Data Acquisition and Control System 4. Bench Tests Performed During System Development a. Bench Test 1 b. Bench Test 2 c. Bench Test 3 d. Bench Test 4 e. Bench Test 5 D. Results E. Conclusion and Future Work F. Acknowledgements G. References APPENDIX A A1. Temperature Control Box (TCB) Wiring A2. Bench Tests A3. Gas Chromatograph (GC) and FTIR Plots APPENDIX B III. A GIS APPROACH TO MONITORING TITAN’S NORTHERN LAKES FOR CHANGE A. Abstract B. Introduction 1. Background C. Methods 1. Shoreline in Titan’s North 2. Transient Feature within an Estuary D. Results 1. Shoreline in Titan’s North 2. Transient Feature within an Estuary E. Discussion F. Conclusion G. References APPENDIX C IV. A GEOLOGICAL CHARACTERIZATION OF LIGEIA MARE IN THE NORTHERN POLAR REGION OF TITAN A. Abstract B. Introduction C. Methods D. Characterization 1. Crater (Location A) 2. Hummocky Terrain (Location B) 3. Peninsula (Location C) 4. River Systems (Location D) 5. Highlands (Location E) 6. Parallel Drainage Channels (Location F) 7. Two Domes (Location G) 8. Low Lying Region (Location H) E. Discussion F. References APPENDIX D APPENDIX E V. CONCLUSION A. Future Work and Further Study APPENDIX F APPENDIX G I. INTRODUCTION This chapter gives an introduction to Saturn's moon Titan, an overview of radar and the use of synthetic aperture radar (SAR) on Titan, the questions this study sought to answer, and an outline for the subsequent chapters. A. SATURN’S MOON TITAN 1. Discovery Saturn has many moons, fifty-three of which have been named to date. One of the more intriguing of these moons is Titan, with its planet-like size, thick nitrogen atmosphere, clouds, lakes, shorelines, riverbeds, and a complex weather system. Since 2004 our knowledge of this body has greatly increased due to data collected by the Cassini-Huygens spacecraft. The decent of the Huygens probe onto Titan’s surface acquired many in situ measurements, and the many close fly-bys of the Cassini orbiter, with its host of remote sensing instruments, continues to supply a wealth of new information which leaves many opportunities to re-characterize the physical properties of this world. Christiaan Huygens (1629-95), who discovered Titan in 1655, was a preeminent Dutch mathematician, physicist, inventor, craftsman, and astronomer. Amongst his many accomplishments, Huygens is credited with developing the wave theory of light, the pendulum clock, making great advances in telescope technology, and hypothesizing that Saturn's varying profile was due to a ring. He designed a state-of-the-art telescope that had an extremely long- focus, with the main lens high up on a pole that utilized pulleys, controlling lines, counterbalances, pointing systems, and had a 50X eyepiece. Along with his brother Constantyn, they developed a machine for grinding and polishing lenses that made use of gears. Using this machine they were able to produce long-focus lenses with far less distortion than lenses polished 1 by hand. Huygens referred to the point of light he saw near Saturn as Luna Saturn – Latin for Saturn’s moon. Huygens discontinued searching for any further moons of Saturn in 1655 when his apparent beliefs in numerology lead him to conclude the solar system’s inventory was complete (Lorenz et al., 2002; Yoder 1988). It’s interesting to wonder what Huygens would have thought of the probe sitting on Titan’s surface that bears his name. The Cassini-Huygens spacecraft entered Saturn's orbit on July 1, 2004, and on December 25, 2004, the Huygens probe was released for its decent to the surface of Titan. The Huygens probe collected 147 minutes, 13 seconds of data during its decent, and 72 minutes, 9 seconds of data while on Titan’s surface. It continued to send data as the Cassini spacecraft disappeared below the horizon (Lebreton et al., 2005). The Cassini orbiter continues to study the Saturnian system. Titan is the second largest moon in the solar system with a diameter of 5150 km. It is second in size only to Jupiter’s moon Ganymede, and is larger than the planet Mercury. Titan is the only solid body beyond Mars with a substantial atmosphere (Rothery 1999). Titan’s average distance from Saturn is 1,221,850 km,